Notes. ^(a) We aim to report the name assigned to a cluster based on its first literature appearance, given a one-to-one relationship and enough similarity between our and the literature selection. For clusters that appear to be contaminated or describe a smaller (noncentral) portion of the disk stream, we also report the name of a more recent study whose extraction aligns better with our findings. This is particularly the case for disk streams S1 and S6, where we have either established a new name (Ratzenboeck 1) or attributed two names to describe the population. ^(b) Literature ages are compiled from the discovery paper and/or follow-up studies with refined membership lists. In cases of very contaminated extractions, we omit the age altogether (see Table C.1). For the open clusters Platais 9 and NGC 2451A, we report the age determined by Bossini et al. (2019); see Meingast et al. (2021) for a more thorough discussion on their fundamental physical parameters across the literature. Here, we report the mean population age rounded to the nearest integer and omit reported uncertainties for easier readability. We refer the reader to the respective source material referenced in the respective “Reference” column for more information. ^(c) Ages listed in the “Literature age” column correspond to the following references: (1) Bossini et al. (2019), (2) Qin et al. (2023), (3) Hunt & Reffert (2023), (4) Kounkel & Covey (2019), (5) Mamajek (2006), (6) Gagné et al. (2018b), (7) Fürnkranz et al. (2024). ^(d) Due to possible contamination, we determine the disk stream lengths not directly from the data but as average peak-to-peak lengths from 100 bootstrap samples, which we report alongside respective standard deviations. ^(e) The disk stream S9 overlaps with the group Theia 301 identified by Kounkel & Covey (2019) who relate it to the AB Doradus moving group. We note here that our selection of S9 is significantly different from Theia 301. While Theia 301 consists of just over 1300 sources, only 188 of them overlap with S9, which itself has over 500 members. Regardless of these differences, we refer to S9 as “Theia 301” throughout this manuscript. ^(f)The disk stream S12 overlaps with the group Theia 599 identified by Kounkel & Covey (2019). Their morphologies and membership lists are similar enough to document a match here. However, we note that the observational HRD and XYZ distribution of Theia 599 indicates substantial field contamination. ^(ɡ) We find significantly nonzero (A_V ≥ 0.1 mag) extinction toward disk streams S1 (A_V = 0.2 mag), S3 (A_V = 0.1 mag), S4 (A_V = 0.1 mag), S8 (AV = 0.5 mag), S11 (A_V = 0.3 mag), S12 (A_V = 0.1 mag). ^(h) We show two estimations of the 3D velocity dispersion. First, the dispersion estimate is derived from the XD procedure. Second, the value in parentheses is determined via the MAD. For more details, see Appendix D.